The oscillation properties of a solar-like oscillator are unambiguously connected to its mass and radius. The simplest and most popular application of asteroseismology consists of comparing the global oscillation propertiesThe oscillation frequency at their maximum amplitude \(\nu _{\mathrm {max}}\)  and the mean frequency spacing \(\Delta \nu \)  between consecutive overtones. of a given star to those of the Sun and retrieving its mass and radius from asteroseismic scaling relations [1]}, [2]}. For RGs, the evolutionary state (hydrogen shell or helium core burning) and core rotation can also be determined from the analysis of the mixed modes, which result from the interaction of gravity (\(g\) ) modes in the radiative core and acoustic pressure (\(p\) ) modes in the convective envelope [3]}, [4]}, [5]}, [6]}, [7]}, [8]}, [9]}, [10]}, [11]}.
